Jets Two classes of jets from X-ray binaries Jet power versus accretion power Jet composition Large-scale jets and interactions with ISM Jet production and collimation
Two Flavors of Radio Jets Compact tens of AU, found in low/hard X-ray state Large scale up to parsecs, produced at state transitions Stirling et al. 2001 High/soft state no jet Mirabel et al. 1994
Compact jets GRS 1915+105 Dhawan et al. (2000) Markoff & Nowak (2004) Small physical size, inverted or flat radio spectra optically thick synchrotron emission from a self-absorbed outflow
Superluminal Motion
Optical Illusion v sin c v cos / c sin =c 1 cos c vτcosθ v obs = v v sin c v cos Seeing two jets gives us two equations to solve for velocity and inclination angle!
What fraction of the total power output of compact objects is in jets versus radiated energy?
Jet from Cygnus X-1 Radio/optical ring near Cyg X-1 serves as calorimeter for jet power. Indicates ratio of jet power to X-ray luminosity is in the range 0.06-1.0. Gallo et al. 2004
TeV emission from LS 5039 TeV from inverse-compton of jet electrons on photons from O6.5V companion or jet protons interacting with stellar wind. TeV luminosity indicates an extremely powerful outflow. For 10% acceleration efficiency, the jet kinetic power must be equal the Xray luminosity. Aharonian et al. 2005
Radio/X-ray Flux Correlation Fradio FX+0.7 Corbel et al. (2000,2003)
Radio/X-ray Flux Correlation Fradio FX+0.7 Corbel et al. (2000,2003)
Jet Domination at Low Accretion Rates Fender et al. 2003 For optically thick jets, the jet power scales as Lradio Ljet0.5 At low accretion rates, this would suggest that the jet power dominates over the X-ray luminosity.
Do the Jets Produce X-Rays?
Are jets electron/proton or electron/positron?
SS 433 Jet discovered via blue/red shifted Balmer emission lines (Margon et al. 1979) Jet extends to scales of 45' (60 pc) (Seward et al. 1980) Large scale jet is non-thermal (Kotani et al. 1994)
SS 433 Optical Spectrum Margon et al. 1979
SS 433 H variations
High-resolution image of SS433
X-rays from the jets ASCA Baryonic Highly ionized Collisional excitation Large temperature and density gradients Chandra
SS 433 inner jet is baryonic and thermal (Migliari et al. 2002)
Questions Are jets re-energized at large distances from origin?
Outbursts of XTE J1550-564 Discovery outburst in 9/1998 Activity in 2000, 2001/2002, 2003. Radio jets in 9/1998 (Hannikainen et al. 2001) Separation speed > 2c.
Large Scale jets of XTE J1550-564 Eastern jet is approaching, western is receding. Corbel et al. 2002, Kaaret et al. 2003
Emission mechanism = 0.66 ± 0.01 Contours = radio, pixels = X-ray Synchrotron emission from single population. Equipartition B ~ 300 G X-ray emitting electrons: e > 2 x107, energy ~ TeV Number electrons ~ 1045 ; if one p/e, mass ~ 1021 g Syncrotron lifetime ~ 10 years
Jet deceleration Approaching jet decelerates gradually. Receding jet brightens only after sharp deceleration. Approaching jet kinetic energy loss rate of 1034 erg/s in June 2000. Luminosity is 1032 erg/s. Need ~ 1% efficiency for conversion of bulk deceleration to particle acceleration. First direct observation of gradual deceleration of BH jet.
Jet/ISM Interactions Appear to have in-situ particle acceleration Deceleration from profile fitted to eastern jet implies kinetic energy loss rate ~ 1034 erg/s in June 2000. Compare to luminosity ~ 1032 erg/s need efficiency of ~ 1% for conversion of bulk deceleration to particle acceleration Mechanism? Internal shocks: internal instabilities, varying flow speed External shocks: interactions with denser ISM
Large scale jet in H1743-322 Outburst starting in March 2003 Radio flare on April 8 Radio rise in ~ 45 days, decay in ~ 30 days
X-ray jets in H1743-322 Eastern jet mid Feb. 04 = 0.65 +/-0.02 p ~ 2.2 E. jet W. Jet Similar properties to the X-ray jets of XTE J1550-564, but decay is much faster (Corbel et al. 2005).
Fossil Jet from 4U 1755-33 Source was active for at least 20 years X-ray jet extends ~ 4 pc Thermal X-ray emission is ruled out Synchrotron is OK TeV electrons B ~ 100 G (Angelini & White 2003; Kaaret et al. 2005) Long lifetime of jet means particles injected into ISM continuously for decades
Jet Production Eikenberry et al. 1998 Simultaneous IR (jet) and X-ray observations of GRS 1915+105 show jet ejection is tightly correlated with rapid disapperance of accretion disk.
Jet Production Cooling of particles in the jets due to adiabatic expansion